|
|
|
|
LEADER |
01460 am a22001933u 4500 |
001 |
112096 |
042 |
|
|
|a dc
|
100 |
1 |
0 |
|a Murphy, K. D.
|e author
|
100 |
1 |
0 |
|a MIT Kavli Institute for Astrophysics and Space Research
|e contributor
|
100 |
1 |
0 |
|a Nowak, Michael A
|e contributor
|
100 |
1 |
0 |
|a Marshall, Herman
|e contributor
|
700 |
1 |
0 |
|a Marshall, Herman
|e author
|
700 |
1 |
0 |
|a Nowak, Michael A.
|e author
|
245 |
0 |
0 |
|a The Nuclear X-Ray Emission-line Structure in NGC 2992 Revealed by
|
260 |
|
|
|b IOP Publishing,
|c 2017-10-31T15:13:08Z.
|
856 |
|
|
|z Get fulltext
|u http://hdl.handle.net/1721.1/112096
|
520 |
|
|
|a We present the narrow emission-line structure revealed by a 135 ks Chandra observation of Seyfert galaxy NGC 2992, using the High Energy Transmission Grating Spectrometer. The source was observed in an historically low-flux state. Using a Bayesian Block search technique, we detected neutral Si Kα and S Kα fluorescence and two additional lines that are consistent with redshifted, ionized Si emission. The latter two features are indicative of a photoionized outflow with a velocity of ∼ 2500 km s⁻¹. We also observed prominent, unresolved line emission at the rest energy of Fe Kα, with a 90% confidence FWHM velocity width of < 2000 km s⁻¹ ( < 2800 km s⁻¹) and equivalent width of 406-1148 eV (288-858 eV) when broad Fe Kα line emission, as detected by Suzaku, was (was not) included in the model.
|
655 |
7 |
|
|a Article
|
773 |
|
|
|t Astrophysical Journal
|